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  The evolution and origin of ionized gas velocity dispersion from z ~ 2.6 to z ~ 0.6 with KMOS3D

Übler, H., Genzel, R., Wisnioski, E., Förster-Schreiber, N. M., Shimizu, T. T., Price, S. H., et al. (2019). The evolution and origin of ionized gas velocity dispersion from z ~ 2.6 to z ~ 0.6 with KMOS3D. The Astrophysical Journal, 880(1): 48. doi:10.3847/1538-4357/ab27cc.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-0FEF-F Version Permalink: http://hdl.handle.net/21.11116/0000-0005-0FF5-7
Genre: Journal Article

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The Evolution and Origin of Ionized Gas Velocity Dispersion from z ~ 2.6 to z ~ 0.6 with KMOS3D.pdf (Any fulltext), 5MB
 
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Übler, H.1, Author              
Genzel, R.1, Author              
Wisnioski, E., Author
Förster-Schreiber, N. M.1, Author              
Shimizu, T. T.1, Author              
Price, S. H.1, Author              
Tacconi, L. J.1, Author              
Belli, S.1, Author              
Wilman, D. J.2, Author              
Fossati, M., Author
Mendel, J. T., Author
Davies, R. L.1, Author              
Beifiori, A., Author
Bender, R., Author
Brammer, G. B., Author
Burkert, A., Author
Chan, J., Author
Davies, R. I., Author
Fabricius, M.2, Author              
Galametz, A., Author
Herrera-Camus, R.1, Author              Lang, P., AuthorLutz, D.1, Author              Momcheva, I. G., AuthorNaab, T., AuthorNelson, E. J., AuthorSaglia, R. P., AuthorTadaki, K., Authorvan Dokkum, P. G., AuthorWuyts, S., Author more..
Affiliations:
1Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159889              
2Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Abstract: We present the 0.6 < z < 2.6 evolution of the ionized gas velocity dispersion in 175 star-forming disk galaxies based on data from the full KMOS3D integral field spectroscopic survey. In a forward-modeling Bayesian framework including instrumental effects and beam-smearing, we fit simultaneously the observed galaxy velocity and velocity dispersion along the kinematic major axis to derive the intrinsic velocity dispersion σ0. We find a reduction of the average intrinsic velocity dispersion of disk galaxies as a function of cosmic time, from σ0 ~ 45 km s−1 at z ~ 2.3 to σ 0 ~ 30 km s−1 at z ~ 0.9. There is substantial intrinsic scatter (δσ 0int ≈ 10 km s−1) around the best-fit σ 0–z relation beyond what can be accounted for from the typical measurement uncertainties (δσ 0 ≈ 12 km s−1), independent of other identifiable galaxy parameters. This potentially suggests a dynamic mechanism such as minor mergers or variation in accretion being responsible for the scatter. Putting our data into the broader literature context, we find that ionized and atomic+molecular velocity dispersions evolve similarly with redshift, with the ionized gas dispersion being ~10–15 km s−1 higher on average. We investigate the physical driver of the on average elevated velocity dispersions at higher redshift and find that our galaxies are at most marginally Toomre-stable, suggesting that their turbulent velocities are powered by gravitational instabilities, while stellar feedback as a driver alone is insufficient. This picture is supported through comparison with a state-of-the-art analytical model of galaxy evolution.

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 Dates: 2019-07-24
 Publication Status: Published online
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 Identifiers: DOI: 10.3847/1538-4357/ab27cc
Other: LOCALID: 3175557
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Title: The Astrophysical Journal
Source Genre: Journal
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Publ. Info: Bristol; Vienna : IOP Publishing; IAEA
Pages: - Volume / Issue: 880 (1) Sequence Number: 48 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215_3